Galaxies A d r i a n o F o n t a n a I N A F - O s s e r v a t o - - PowerPoint PPT Presentation

(Clues on) The Origin of Massive Galaxies

A d r i a n o F o n t a n a

I N A F - O s s e r v a t o r i o A s t r o n o m i c o d i R o m a M . C a s t e l l a n o , S . C r i s t i a n i , F . F i o r e , E . G i a l l o n g o , N . M e n c i , M . N o n i n o , L . P e n t e r i c c i , S . S a l i m b e n i , P . S a n t i n i , E . V a n z e l l a

VLT: U+JHK HST: BVIz Spitzer:IRAC (3.5-8µm) Spitzer: MIPS 24µm

4000 K<23.5 galaxies 10000 z<6 galaxies >1000 spectroscopic z+ well calibrated zphot (UV+24µm)-to-SFR relations from Papovich+07, Daddi +07 etc GOODS-South: the GOODS-MUSIC sample

(Grazian +06, http://lbc.oa-roma.inaf.it/goods)

1) Fundamental Cosmology: the density of massive galaxies as compared with the expected density

• f DM haloes;

2) Tests and constraints on galaxy formation models in a ΛCDM Universe: Stellar masses and SFRs are the most straightforward outputs of such models

Pozzetti+ 07

1) Fundamental Cosmology: the density of massive galaxies as compared to the expected density of DM haloes;

Rodighiero + 07 Fontana + 04 (see also Pozzetti +07)

Fontana+ 06

2) Tests and constraints on galaxy formation models in a ΛCDM Universe: Density of massive galaxies is 50% at z=1.5-2 Much faster evolution of massive galaxies at z>2

Massive galaxies at high z: a test for “ab initio” theoretical models? Not a critical one (anymore)...OK within systematics What are the physical properties of the objects that contribute to the steep rise at z>2? Are they reproduced by the models?

Kitzbichler&White 07

Menci+06

Menci+06

Millennium simulation “radio mode”AGN feedback Semianalytic rendition “bright QSO phase” feedback

How to build up a homogeneous sample of red galaxies, complete in mass and redshift, discriminating between Star Forming and Passively Evolving? SED fitting Classification of 80% of the

• bjects is independent of the

details of SFRH and photo-z uncertainites E(B-V)=0.03 Age = 2.5 Gyr τ = 0.1 Gyr E(B-V)=0.9 Age = 0.15 Gyr τ = 1 Gyr

z≈2

Similar to many color selection criteria: (I-K)/(J-K) (Pozzetti& Mannucci 00) BzK (Daddi+04) (U-V)/(V-J)(Wuyts+06)

The contribution of Star Forming and Passively Evolving galaxies to the mass budget of the Universe Passively evolving galaxies show a strong negative evolution from z~2 to z~3.

Grazian +07

Quantitative use of the 24 micron photometry The 24mm/K flux ratio as SED indicator

Empirical UV-to-MidIR SED (Polletta+06)

The 24 micron vs SED fitting The criterion based on SED fitting is in agreement with 24µm/K flux ratio.

Candidate Obscured AGNs Fiore +07 (see also Daddi+07)

A sizeable fraction of galaxies is already in a quiescent phase at z~2. “Robust” candidates of “Red&Dead” galaxies at z>2.5

Final step: convert the observational criteria into a physical criteria --> comparison with models.

M > 5E10 Msun

Stellar Mass / SFR

SFR estimated as in Papovich+07, Daddi+07

criterion#1 D.T. > 1E11 yr --> “Quiescent” galaxies criterion#2 D.T. < Universe Age(z) --> “Active” galaxies

Comparison of GOODS-MUSIC data with Millennium Simulation

“Active” “Quiescent”

1 2 3 4 0.2 0.4 0.6 0.8 1 1 2 3 4 0.2 0.4 0.6 0.8 1

The Millennium Simulation seems to underpredict the “active fraction” due to an underprediction of the average SFR, while overpredicting the Mass Density Too much action moved at higher redshift and/or into smaller progenitors?

Kitzbichler&White 07

Summary & Conclusions

1) Constraints on fundamental DM statistics: passed 2) The epoch z>=2 is a major phase in the assembly of massive galaxies;

• Strong evolution of the stellar mass density at z>2 (50% local)
• Emergence of the red sequence from z=3.5 to z=2;

3) “Red & Dead” galaxies exist up to z=3 and most likely above: need for efficient feedback/quenching of SFR mechanisms at high z 4) At z>=2, about 50% of massive galaxies are experiencing a major peak in their SFRH: during this process they accrete a substancial fraction of their mass (see also Daddi+07) 5) The Millennium simulation seems to underpredict the “active fraction” due to an underprediction of the average SFR, while overpredicting the Mass Density: to quench SF and prevent overcooling in massive galaxies, too much action moved at higher redshift and/or smaller progenitors? Comparison with

• ther models on the way.